Using Monte Carlo techniques, we calculate the bremsstrahlung spectrum that protons and electrons in the solar wind would produce when encountering dark matter (DM) particles within the solar system. We consider two types of interactions for the DM: one where a spin-<a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mrow><a:mn>1</a:mn><a:mo>/</a:mo><a:mn>2</a:mn></a:mrow></a:math> neutral DM particle interacts with matter through the exchange of a lighter neutral scalar DM particle and one where a scalar neutral DM particle interacts directly with the matter particle. We consider three wavelengths: 21 cm, 3 mm, and <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:mrow><c:mn>12</c:mn><c:mtext> </c:mtext><c:mtext> </c:mtext><c:mi mathvariant="normal">μ</c:mi></c:mrow></c:math>. To estimate the significance of the signal, we compare our results to experimental results from ARCADE2 and PLANCK and consider the sensitivities of three telescopes: VLA, ALMA, and KECK. We find that in order to produce an observable signal in the first scenario the neutral fermion must have a mass comparable to the solar wind particle while the exchanged particle must have a mass typically <f:math xmlns:f="http://www.w3.org/1998/Math/MathML" display="inline"><f:mrow><f:mi>few</f:mi><f:mo>×</f:mo><f:msup><f:mrow><f:mn>10</f:mn></f:mrow><f:mrow><f:mn>5</f:mn></f:mrow></f:msup></f:mrow></f:math> smaller. The scalar direct interaction, however, appears beyond reach for any reasonable coupling. 

Solar wind bremsstrahlung off dark matter in our solar system at three wavelengths

We consider the possibility that the solar wind emits photons via bremsstrahlung when colliding with dark matter particles within the Solar System. To this effect, we calculate the bremsstrahlung spectrum that a proton would emit when colliding with a neutral spin-$1/2$ particle through the exchange of a scalar neutral particle. We assume a speed of $600\text{ }\text{ }\mathrm{km}/\mathrm{sec}$ for the solar wind and assume that the speed of the dark matter halo is due to the motion of the Sun through our Galaxy, which we take as $300\text{ }\text{ }\mathrm{km}/\mathrm{sec}$. We assume a dark matter density of $0.3\text{ }\text{ }\mathrm{GeV}/{\mathrm{cm}}^{3}$ and a solar wind composed primarily of protons with a total rate of ejection mass set at ${10}^{9}\text{ }\text{ }\mathrm{kg}/\mathrm{sec}$. We use a Monte Carlo technique to let this interaction take place within the Solar System and calculate the photon rate an observer would detect on Earth or at the edge of the Solar System as a function of photon energy. We find that the rates are in general very small but could be observable in some scenarios at wavelengths in the mm range at a telescope like ALMA; this could lead to interesting constraints on couplings and masses. 

Solar wind bremsstrahlung off dark matter in our Solar System

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Solar wind bremsstrahlung off dark matter in our Solar System